matteo guainazzi science operations & data systems division research & scientific support...

Matteo GuainazziMatteo GuainazziScience Operations & Data Systems Division

Research & Scientific Support Department“Stellar-mass, intermediate-mass and supermassive black holes” –Kyoto (Japan) – 28-31 October 2003

XMM-NewtonXMM-Newton

A time(scales) trip to Mkn478A time(scales) trip to Mkn478with XMM-Newtonwith XMM-Newton

Matteo GuainazziMatteo Guainazzi

XMM-Newton Science Operations CenterXMM-Newton Science Operations Center

Research and Science Support Division of ESA, Research and Science Support Division of ESA,

VILSPA, SpainVILSPA, Spain

J.Clavel, N.Loiseau, A.Orr (ESA), F.Fiore (Oss. Monteporzio)J.Clavel, N.Loiseau, A.Orr (ESA), F.Fiore (Oss. Monteporzio)

K.Mason, E.Puchnarewicz (MSSL), G.Matt, G.C.Perola (Un. Roma Tre),K.Mason, E.Puchnarewicz (MSSL), G.Matt, G.C.Perola (Un. Roma Tre),




GoalGoal

Narrow Line Seyfert 1 Galaxies are X-ray variable Narrow Line Seyfert 1 Galaxies are X-ray variable [talk T.Boller][talk T.Boller]

Their X-ray spectra have two-components, directly Their X-ray spectra have two-components, directly related to accretion related to accretion [posters C.Matsumoto, M.Murashima][posters C.Matsumoto, M.Murashima]

XMM-Newton covers the XMM-Newton covers the whole 0.1-10 keV whole 0.1-10 keV with with unprecedented sensitivity unprecedented sensitivity (RXTE: 2-20 keV)(RXTE: 2-20 keV)

design a specific experiment to probe the spectral variability in design a specific experiment to probe the spectral variability in NLSy1s on a range of different timescalesNLSy1s on a range of different timescales




Important timscales for AGNImportant timscales for AGN

Light crossing time Light crossing time (M(MBHBHMM77101077 M Msunsun RRRRgg)) lclc 200 200 M M7 7 secondsseconds

Keplerian flow dynamic timescaleKeplerian flow dynamic timescale KK 15 15 3/23/2 M M7 7 minutesminutes

Thermal timescale thth -1-1 KK hourshours

Viscous timescaleViscous timescale vv thth (r/h) (r/h)2 2 days/monthsdays/months

Disk reprocessing/torus reprocessing/diffuse Disk reprocessing/torus reprocessing/diffuse gas ...gas ...

h

r




The Mkn478 monitoring programThe Mkn478 monitoring program

Why Mkn478?Why Mkn478?– VariableVariable– Weak reprocessing featuresWeak reprocessing features– Low absorptionLow absorption

– NH,Gal=1.01020 cm-2

Which data?Which data?– 1 ASCA observation 1 ASCA observation (July 1995)(July 1995)– 1 BeppoSAX observation 1 BeppoSAX observation (Aug 2000)(Aug 2000)– 1 XMM-N observation 1 XMM-N observation (Dec 2001)(Dec 2001)– 3 close XMM-N observations 3 close XMM-N observations (1, (1,

4, 7 Jan 2003)4, 7 Jan 2003)– Exposure times:

– 30 ks (ASCA)– 50 ks (BeppoSAX)– 20 ks (XMM-N)

(Leighly 1999)

Mkn478

Mkn478 is a micro-cosmos ofNarrow Line Seyfert 1 variability




XMM-Newton spectraXMM-Newton spectra

Double power-law fitsSOFT BAND HARD BAND

E=6.700.08 keVEW=12080 eVP96%




The history of the X-ray SED in Mkn478The history of the X-ray SED in Mkn478

Flux dynamical ranges:Flux dynamical ranges:– 2 in soft X-rays2 in soft X-rays– 4 in hard X-rays4 in hard X-rays

Constant soft X-ray Constant soft X-ray spectral shapespectral shape Variable hard X-ray Variable hard X-ray spectral shape (spectral shape (1.0)1.0)

– No correlation with the No correlation with the soft, hard or total X-ray soft, hard or total X-ray powerpower

Soft/hard X-ray Soft/hard X-ray luminosity ratio luminosity ratio 0.4-2.50.4-2.5




(Lack of) spectral correlations(Lack of) spectral correlations

soft vs. Fsodthard vs. Fhard

RLsoft/Lhard vs. FX

vs. R

(Haardt et al. 1997)

Expected tracks for a pair-dominatedplasma: face-on disk and Tbb = 100 eV




The The quest for the “quest for the “physical driverphysical driver””

kT0=60 eV

2001: kT0=683 eV2003: kT0=58.51.9 eV

Double Comptonization scenario(Titarchuck & Lyubarskij 1994, Hua & Titarchuck 1994)




Variablity on shorter timescalesVariablity on shorter timescales

0.2-1 keV

3-10 keV




The quest for the “typical” variability timescaleThe quest for the “typical” variability timescale

Structure function:SF() = < [ F(t) - F(t+) ]2 >

(Simonetti et al. 1985)

Normalized excess variance2

nxs = (2obs- 2

exp)/<x>2

(Na

nd

ra e

t a

l . 1

99

7,

Ed

els

on

et

al.

20

02

, V

au

gh

an

et

al .

20

03

)

0.6




Spectral variability between bandsSpectral variability between bands

Cro

ss-c

orr

elat

ion

0.2

-1 k

eV v

ersu

s 3-

10 k

eV

Jan 7 – 1st half

Jan 7 – 2nd halfHar

dn

ess

rati

o 0

.2-1

keV

ver

sus

3-10

keV

R 0.9same soft

same hard




Spectral variabilty in the soft bandSpectral variabilty in the soft band




Spectral variability in the hard bandSpectral variability in the hard band

HR vs count ratecorrelation probabilities:

P 50% P 82% P 95%

“Flares” light curve and HR




SummarySummary

The hard X-ray The hard X-ray fluxflux varies varies achromaticallyachromatically on timescales of on timescales of fraction of hoursfraction of hours

The hard X-ray The hard X-ray spectrumspectrum varies on timescales of varies on timescales of daysdays, with no , with no obvious correlation with the X-ray powerobvious correlation with the X-ray power

No unique physical driver for the long-term variabilityNo unique physical driver for the long-term variability The soft X-ray The soft X-ray fluxflux varies varies almost achromaticallyalmost achromatically on scales of on scales of

hours to dayshours to days Soft and hard X-rays are related – by not Soft and hard X-rays are related – by not corcorrelated – on related – on

scales of scales of hours hours driven by a common physical parameter? driven by a common physical parameter?– On longer timescales this relation is basically lostOn longer timescales this relation is basically lost

The scenario is complex:The scenario is complex:– careful selection of the energy bands to study is crucialcareful selection of the energy bands to study is crucial– different timescales mixdifferent timescales mix




EndEnd

Lunch timeLunch time




Recent results on Seyfert variabilityRecent results on Seyfert variability

(Page et al. 2002)

(Gallo et al. 2003)(Gliozzi et al. 2001)

(Pe

tru

cci e

t a

l. 20

03

)

IRAS13224-3809

PKS0558-504

1H0419-577

NGC7469




Multi-blackbody modelsMulti-blackbody models

kT 70 eV

kT 120 eV

kT 1700 eVkT 50 eV

kT 120 eV

kT 250 eV

kT 50 eV

kT 100 eVkT 200 eV

kT 75 eV

kT 210 eV

kT 1700 eV




Narrow-band featuresNarrow-band features

OVII

In 7-Jan-2003 observation only:the lowest hard X-ray flux everlowest hard X-ray flux ever

E=6.700.09 keVEW=12080P(F-test)96.7

Photoabsorption edge?

matteo guainazzi science operations & data systems division research & scientific support...

Documents

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